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The study aims to analyze far-ultraviolet emission lines from T Tauri stars to understand their molecular processes and outflows.

February 20, 2002The Astrophysical JournalOpen Access

Observations of T Tauri Stars usingHubble Space TelescopeGHRS. I. Far‐Ultraviolet Emission Lines

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Observations of far-ultraviolet emission lines in T Tauri stars provide insights into molecular outflows and accretion processes.

The study aims to analyze far-ultraviolet emission lines from T Tauri stars to understand their molecular processes and outflows.
Analyzed GHRS data of eight classical T Tauri stars (CTTS) and one weak T Tauri star (WTTS).
Measured spectral ranges centered on key wavelengths (1345, 1400, 1497, 1550, and 1900 Å).
Assessed column densities and optical depths of H2 emission lines and analyzed excitation routes.
Observed strong SiIV and CIV emission with widths of ~200 km/s and blueshifted line centroids.
Identified H2 emission lines as products of fluorescence due to Ly_alpha excitation, indicating molecular outflows.
Noted that while CIV is typically optically thin, SiIV is not, although CIV can predict H2 and SiIV emissions effectively.

Ardila et al. (2002) studied this question.

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